E. Khomenko and M. Collados

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Presentation transcript:

E. Khomenko and M. Collados EFFECTS OF PARTIAL IONIZATION IN THE PHOTOSPHERE AND IN THE CHROMOSPHERE E. Khomenko and M. Collados

Approximation of magnetohydrodynamics + Fully ionized Coupled by collisions Single fluid description

photosphere chromosphere

Approximation of magnetohydrodynamics Multi-fluid approximation + B + Fully ionized Coupled by collisions Single fluid description Weakly ionized Less coupled by collisions Sunspots and chromosphere Best valid in the deep photosphere and convection zone

Equations of Magnetohydrodynamics

Equation for individual species

Combined quasi-MHD equations

Diffusivities

Conversion of magnetic to thermal energy

Z = 1000 km 900 G 750 G 600 G 450 G 300 G

Z = 1000 km

Conclusions Collissions with neutrals (ambipolar diffusion) can lead to a significant temperature rise (~ 2000 k) within minutes at chromospheric level Important plasma motions can appear during the heating process

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